As shown in GR simulations[1]} the ejected mass in a violent BNS merger is mostly stripped from the inner and outer crust of the NSs and will be determined by the energetics of the collision and the actual amount of matter in the crust. In a NS the neutron rich crust displays a large set of inhomogenous substructures ranging from lattice nuclei to pasta phases [2]}. In the thin-crust approximation \(M_{\rm {crust }} \approx \frac{4 \pi R^{3} P_{t}}{c^2 C}[1-2 C]\)  where \(P_t\)  is the EoS dependent pressure transition from the crust-core regions [3]}. There is a large sensitivity to the EoS in the crust mass value, being smaller for heavier stars. Recent Bayesian analysis[4]} provide values for the transition density \(n_t = 0.072\pm 0.011\)  \(\rm fm^{-3}\)  and the transition pressure \(P_t = 0.339\pm 0.115\)  \(\rm MeV\)  \(\rm fm^{-3}\) . The resulting crust masses \(M^{\rm DD2}_{\rm {crust }}=0.038M_\odot \)  and \(M^{\rm SFHo}_{\rm {crust }}=0.024M_\odot \) . In addition, the number of baryons must be conserved \(N^*_1+N^*_2=N^*_{remnant}+N^*_{ejec}\) .
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